The spectrum of solar cosmic rays: Data of observations and numerical simulation

Spectrum of solar flare protons

“…The measured and calculated spectra are coincident, if the rate of reconnection in the numerical experiment is $ 10 7 cm=s. The delayed component of flare relativistic protons shows a power law spectrum $ W Àg with g $ 5 (Vashenyuk et al, 2003(Vashenyuk et al, , 2006Balabin et al, 2005). There is a temptation to explain the delayed component by particle acceleration in a shock created by the coronal mass ejection (Dryer, 1996).…”

“…The delayed component shows the power law spectrum dI=dW ¼ BW g with g ¼ 5. Both parameters W 0 ¼ 0.5 GeV and g $ 5 are typical for most of the flares (Vashenyuk et al, 2003;Balabin et al, 2005).…”

“…However, the potential magnetic field with an X-type singular line and the constant electric field along it used by Balabin et al (2005) is only a rough approximation to magnetic and electric field distributions in a flare current sheet. It is necessary to calculate the spectrum in the current sheet for a real flare.…”

“…If the relation between proton flux on the magnetospheric boundary and monitor reaction is known, any station of the world net can be considered as a unit of the multidirectional energy analyzer of solar cosmic rays. The results of measurements with neutron monitors provide information about the spectrum of relativistic protons in the energy range up to 20 GeV (Vashenyuk et al, 2003;Balabin et al, 2005).…”

Solar flares dynamics investigation using UV diagnostics

“…A similar mechanism of proton accelerate has been observed in the laboratory studies of a powerful pulsed gas discharge (Artsimovich, 1958). Protons with the energy of ~ 20 GeV accelerated in a solar flare are demonstrated with the worldwide network of neutron monitors (Balabin et al, 2005;Podgorny at al., 2010a;2010b). This result gives us hope to get new information about the mechanism of galactic cosmic rays generation.…”